$\begin{figure} \par\includegraphics[width=7.4cm,clip]{H4509F6.eps} \end{figure}$ Figure 2: Time evolution of Sa model spectra for ages 1, 3, 6 and 12 Gyr (bottom to top). Fluxes are in units of erg cm^-2 s^-1 Å^-1, wavelength in Å.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{H4509F7.eps}\par\includegraphics[width=7.1cm,clip]{H4509F8.eps} \end{figure}$ Figure 3: Relative luminosity contributions to U, V, K bands from stellar subpopulations of various metallicity for 12 Gyr old E (top) and Sb (bottom) model.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{H4509F9.eps} \end{figure}$ Figure 4: Relative luminosity contributions to U, V, K bands from stellar subpopulations of various metallicity for a 6 Gyr old Sb model.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4509F10.eps}\par\includegraphics[width=7.2cm,clip]{H4509F11.eps} \end{figure}$ Figure 5: Time evolution of the luminosity contribution to the V-band of the different metallicity subpopulations to the total luminosity for the E (top) and Sb (bottom) models.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4509F18.eps}\par\includegraphics[width=7.2cm,clip]{H4509F19.eps} \end{figure}$ Figure 8: Comparison of cc and ${Z_{\odot }}$ models for Sb in the U-, B-, and K-band. Decomposition into evolutionary (top) and cosmological (bottom) corrections.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{H4509F21.eps}\par\vspace*{2mm} \includegraphics[width=8.1cm,clip]{H4509F22.eps} \end{figure}$ Figure 10: Comparison between our cc models and the solar models of Poggianti (1997) (P). The top panel shows the k-corrections and the bottom panel the e-corrections for E and Sc models in U. Note that we compare none-attenuated models in Poggianti's cosmology $(H_0,\Omega_0)=(50,~0.5)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{H4509F25.eps}\par\vspace*{2mm} \includegraphics[width=8.2cm,clip]{H4509F26.eps} \end{figure}$ Figure 12: Redshift evolution of B-band luminosity (m450) and from the B-V colour (m450-m606) compared to the HDF galaxies photometric redshift catalogue of Sawicki et al. (1997). Vertical bars show the $1\sigma$ luminosity and colour ranges of local galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{H4509F1.eps}\par\includegr... ...p]{H4509F4.eps}\par\includegraphics[width=6.5cm,clip]{H4509F5.eps} \end{figure}$	Figure 1: Comparison of our model spectra (solid) at an age $T{_{\rm gal}}\sim 12$ Gyr (E, Sa, Sb, Sc) and $T{_{\rm gal}}\sim 4$ Gyr (Sd) with Kennicutt's template spectra (dotted).
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{H4509F6.eps} \end{figure}$	Figure 2: Time evolution of Sa model spectra for ages 1, 3, 6 and 12 Gyr (bottom to top). Fluxes are in units of erg cm^-2 s^-1 Å^-1, wavelength in Å.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{H4509F7.eps}\par\includegraphics[width=7.1cm,clip]{H4509F8.eps} \end{figure}$	Figure 3: Relative luminosity contributions to U, V, K bands from stellar subpopulations of various metallicity for 12 Gyr old E (top) and Sb (bottom) model.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{H4509F9.eps} \end{figure}$	Figure 4: Relative luminosity contributions to U, V, K bands from stellar subpopulations of various metallicity for a 6 Gyr old Sb model.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4509F10.eps}\par\includegraphics[width=7.2cm,clip]{H4509F11.eps} \end{figure}$	Figure 5: Time evolution of the luminosity contribution to the V-band of the different metallicity subpopulations to the total luminosity for the E (top) and Sb (bottom) models.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4509F12.eps}\par\includeg... ...{H4509F13.eps}\par\includegraphics[width=7.2cm,clip]{H4509F14.eps} \end{figure}$	Figure 6: Time evolution of the luminosity-weighted stellar metallicities in U, V, and K (restframe) for different spectral types E, Sb, Sd (top to bottom).
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{H4509F15.eps}\par\includeg... ...{H4509F16.eps}\par\includegraphics[width=6.6cm,clip]{H4509F17.eps} \end{figure}$	Figure 7: Comparison of the (e+k) corrections in cc and ${Z_{\odot }}$ models for E (top), Sb (middle) and Sd (bottom) galaxies in U, B and K band ${(H_0,~\Omega_0) ~=~ (65,~0.1)}$ .
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4509F18.eps}\par\includegraphics[width=7.2cm,clip]{H4509F19.eps} \end{figure}$	Figure 8: Comparison of cc and ${Z_{\odot }}$ models for Sb in the U-, B-, and K-band. Decomposition into evolutionary (top) and cosmological (bottom) corrections.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{H4509F20.eps} \end{figure}$	Figure 9: K-correction - including the attenuation - for the Sb-model.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{H4509F21.eps}\par\vspace*{2mm} \includegraphics[width=8.1cm,clip]{H4509F22.eps} \end{figure}$	Figure 10: Comparison between our cc models and the solar models of Poggianti (1997) (P). The top panel shows the k-corrections and the bottom panel the e-corrections for E and Sc models in U. Note that we compare none-attenuated models in Poggianti's cosmology $(H_0,\Omega_0)=(50,~0.5)$ .
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{H4509F23.eps}\par\vspace*{2mm} \includegraphics[width=8.2cm,clip]{H4509F24.eps} \end{figure}$	Figure 11: Same like Fig. 10, but now in the B-band.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{H4509F25.eps}\par\vspace*{2mm} \includegraphics[width=8.2cm,clip]{H4509F26.eps} \end{figure}$	Figure 12: Redshift evolution of B-band luminosity (m450) and from the B-V colour (m450-m606) compared to the HDF galaxies photometric redshift catalogue of Sawicki et al. (1997). Vertical bars show the $1\sigma$ luminosity and colour ranges of local galaxies.
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